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The survival of asteroid Vesta during the violent early history of the SolarSystem is a pivotal constraint on theories of planetary formation. Particularlyimportant from this perspective is the amount of olivine excavated from thevestan mantle by impacts, as this constrains both the interior structure ofVesta and the number of major impacts the asteroid suffered during its life.The NASA Dawn mission revealed that olivine is present on Vesta's surface inlimited quantities, concentrated in small patches at a handful of sites andinterpreted as the result of the excavation of endogenous olivine. Later worksraised the possibility that the olivine had an exogenous origin, based on thegeologic and spectral features of the deposits. In this work we quantitativelyexplore the proposed scenario of a exogenous origin for the detected olivine toinvestigate whether its presence on Vesta can be explained as a natural outcomeof the collisional history of the asteroid. We took advantage of the impactcontamination model previously developed to study the origin and amount of darkand hydrated materials observed by Dawn on Vesta, which we updated byperforming dedicated hydrocode impact simulations. We show that the exogenousdelivery of olivine by impacts can offer a viable explanation for the currentlyidentified olivine-rich sites without violating the constraint posed by thelack of global olivine signatures on Vesta. Our results indicate that no mantleexcavation is in principle required to explain the observations of the Dawnmission and support the idea that the vestan crust could be thicker thanindicated by simple geochemical models based on the Howardite-Eucrite-Diogenitefamily of meteorites.

Olivine on Vesta as exogenous contaminants brought by impacts: Constraints from modeling Vesta's collisional history and from impact simulations